Advisors: Jiong Qiu and Dana Longcope
Solar flares are spectacular energy release events in the Sun's atmosphere. It is understood that the energy to fuel flares is provided by the Sun's magnetic fields, most probably through a physical process called magnetic reconnection. Magnetic reconnection changes the way magnetic field lines connect to the Sun's surface, and the subsequent energy release is often manifested as heating along a multitude of newly formed magnetic flux tubes. Magnetic reconnection may also form large scale structures called flux ropes.
In this project, we will analyze solar flare observations to measure properties of magnetic reconnection, such as the total amount of magnetic flux in reconnection, and the rate and geometry of reconnection. These parameters, aided with models, will help us understand how released magnetic energy is used to heat flare plasmas, and how magnetic field is re-organized by reconnection. Student will analyze solar flare images and radiation light curves taken in ultraviolet and extreme-ultraviolet wavelengths by the satellite Solar Dynamic Observatory. Student will learn about the Sun's atmosphere and magnetism. Experience with IDL or similar programming languages is desired though not required.
You can read about related REU projects here: http://solar.physics.montana.edu/home/www/reu/2012/sturrock/